提高电铸局部电沉积速率试验研究

电铸成型是采用离子沉积的方法制造复制件，具有很好的复制精度，因此电铸技术得到了广泛的应用。但由于受极限电流密度等多方面因素的影响，电铸速率一直是制约电铸技术发展的一个瓶颈，许多学者为此做了大量的理论和试验研究，但对如何提高极限电流密度还没有提供一个比较满意的答案，为提高电铸局部电沉积速率，本文在前人工作的基础上，讨论了影响电铸速率的因素，提出了一种新型的电铸方法－喷射式电铸，并通过两组试验分析了局部电沉积速率怀电铸液流量的关系以及局部铸速率与喷嘴口径的关系，试验结果表明，采用喷射式电铸可以大大提高局部极限电流密度，从而使电铸局部电沉积速率有一个较大范围的提高，为将电铸与快速成型结合奠定了试验基础。     

铝蒙皮涂装施工用的水溶性脱漆剂

本文研究的是以苯甲醇替代二氯甲烷为主溶剂的水溶性脱漆剂，它和传统的二氯甲烷型脱漆剂相比，毒性更小、对使用者的安全及身体健康元不利影响，且脱漆速度相当。通过对脱漆剂使用的研究和对比，结果证明，它对环氧类涂料、环氧锌黄底漆等都适用，尤其对于飞机蒙皮漆有良好脱漆效果。该脱漆剂具有原材料易得、对基才腐蚀性小、适用范围广、不燃烧等特点，一般常温下在30分钟内使可将漆膜溶胀。其与制工艺简单，涂覆方便、不易挥发、贮存较稳定，重涂性能好，对基村的后处理无不良影响。     

尾流作用下对转涡轮叶片振动的流固耦合数值分析

采用对转涡轮设计可以提高喷气发动机的推重比.本文应用ANSYS/CFX软件,采用流固耦合数值分析方法对低压涡轮转子叶片进行了分析.对一定的涡轮工况,得到了高压涡轮转子叶片尾流作用下的低压涡轮转子叶片振动的应力和变形变化规律.采用傅里叶变换,对流体激励力、叶片应力及变形相应进行频谱分析,结果表明:在复杂来流激励下,叶片的第一阶振动较易被激起;但高阶振动响应不可忽略;而且叶身温度场不同,被激起的振动阶次也不同.     

多孔复合微结构的制备与减反射性能

主要研究了多孔-金字塔和多层多孔-金字塔两种多孔复合微结构的减反射性能。多孔-金字塔是将带有金字塔结构的单晶硅片置于HF/Fe(NO3)3溶液中二次化学腐蚀得到的,而多层多孔-金字塔复合微结构是将带有金字塔结构的单晶硅片置于HF/CH3CH2OH溶液中二次电化学腐蚀得到的。用扫面电镜和UV-vis-NIR分光光度计分别分析了这两种复合结构的表面形貌和反射率。结果表明,在400~800 nm波长范围内,多孔-金字塔和多层多孔-金字塔复合微结构的平均反射率分别为5%和2.1%。多孔-金字塔微结构表面的孔洞较大,表面的金字塔有少量的塌陷,但多层多孔-金字塔微结构表面的孔洞细小且覆盖均匀,表面的金字塔基本上保持完好。通过比较,电化学方法制备的多层多孔-金字塔复合微结构的减反射效果要优于采用化学腐蚀制备的多孔-金字塔复合微结构的减反射效果。     

Dynamics of Planetary Waves in the Ionosphere as Observed from GPS Satellites

The GPS satellite data are used to study the dynamics of the ionospheric total electron content (TEC) over Central Europe in the summer season from June 23 to September 30, 1996. The TEC variations within the range of periods typical of the planetary waves were found to be nearly synchronous with the neutral wind variations in the mesosphere and with the variations in the occurrence of ionospheric sporadic layers. The observed TEC variations were interpreted as the result of penetration of energy carried by nonstationary Rossby waves to the upper atmospheric altitudes.     

A statistical study of C IV regions in 20 Oe-stars

In this paper, using the Gauss-Rotation model (GR model), we analyse the UV C IV resonance lines in the spectra of 20 Oe-stars of different spectral subtypes, in order to detect the structure of C IV region. We study the presence and behavior of absorption clouds and analyse their characteristics. From this analysis we can calculate the values of a group of physical parameters, such as the apparent rotational and radial velocities, the random velocities of the thermal motions of the ions, the Full Width at Half Maximum (FWHM), the optical depth, as well as the absorbed energy and the column density of the independent regions of matter, which produce the main and the satellite clouds of the studied spectral lines. Finally, we present the relations between these physical parameters and the spectral subtypes of the studied stars and we give our results about the structure of the C IV region in their atmosphere.     

Latitudinal variation of the topside electron temperature at different levels of solar activity

A database of electron temperature (T_e) measurements comprising of most of the available satellite measurements in the topside ionosphere is used for studying the solar activity variations of the electron temperature T_e at different latitudes, altitudes, local times and seasons. The T_e data are grouped into three levels of solar activity (low, medium, high) at four altitude ranges, for day and night, and for equinox and solstices. We find that in general T_e changes with solar activity are small and comparable in magnitude with seasonal changes but much smaller than the changes with altitude, latitude, and from day to night. In all cases, except at low altitude during daytime, T_e increases with increasing solar activity. But this increase is not linear as assumed in most empirical T_e models but requires at least a parabolic approximation. At 550 km during daytime negative as well as positive correlation is found with solar activity. Our global data base allows to quantify the latitude range and seasonal conditions for which these correlations occur. A negative correlation with solar activity is found in the invdip latitude range from 20 to 55 degrees during equinox and from 20 degrees onward during winter. In the low latitude (20 to −20 degrees invdip) F-region there is almost no change with solar activity during solstice and a positive correlation during equinox. A positive correlation is also observed during summer from 30 degrees onward.     

Survival and death of the haloarchaeon Natronorubrum strain HG-1 in a simulated martian environment

Halophilic archaea are of interest to astrobiology due to their survival capabilities in desiccated and high salt environments. The detection of remnants of salty pools on Mars stimulated investigations into the response of haloarchaea to martian conditions. Natronorubrum sp. strain HG-1 is an extremely halophilic archaeon with unusual metabolic pathways, growing on acetate and stimulated by tetrathionate. We exposed Natronorubrum strain HG-1 to ultraviolet (UV) radiation, similar to levels currently prevalent on Mars. In addition, the effects of low temperature (4, −20, and −80 °C), desiccation, and exposure to a Mars soil analogue from the Atacama desert on the viability of Natronorubrum strain HG-1 cultures were investigated. The results show that Natronorubrum strain HG-1 cannot survive for more than several hours when exposed to UV radiation equivalent to that at the martian equator. Even when protected from UV radiation, viability is impaired by a combination of desiccation and low temperature. Desiccating Natronorubrum strain HG-1 cells when mixed with a Mars soil analogue impaired growth of the culture to below the detection limit. Overall, we conclude that Natronorubrum strain HG-1 cannot survive the environment currently present on Mars. Since other halophilic microorganisms were reported to survive simulated martian conditions, our results imply that survival capabilities are not necessarily shared between phylogenetically related species.     

火星磁层顶形成和变化的理论研究

考虑太阳风动压与行星电离层中的带电粒子热压及磁压之和平衡,建立了有大气（电离层）的行星磁层顶形成的理论模型,结合卫星对火星的观测数据,对子午面内向日侧火星磁层顶位形进行了数值计算和分析,研究了火星磁层顶位形及其与太阳风动压之间的变化关系．结果认为,火星磁层顶位形与地球磁层顶相似．太阳风动压越大,火星磁层顶越靠近火星;太阳风动压越弱,火星磁层顶越远离火星．根据火星内秉磁矩从古到今逐渐减小的观点,探索了大尺度磁场（内禀磁矩）对火星磁层顶的贡献作用,结果认为大尺度磁场越强,火星磁层顶越远离行星．这对于进一步研究火星磁层的长期演化以及其他行星磁层的位形变化都具有重要的意义．     

The origin of the prompt optical emission in GRB 060111B

The detection of a bright optical emission measured with good temporal resolution during the prompt phase makes GRB 060111B a rare event that is especially useful for constraining theories of the prompt optical emission. Comparing this burst with other GRBs with evidence of optical peaks, we find that the optical peak epoch (t_p) is anti-correlated with the high energy burst energetic assuming an isotropic energy release (E_iso) in agreement with Liang et al. (2009), and that the steeper is the post-peak afterglow decay, the less is the agreement with the correlation. GRB 060111B is among the latters and it does not match the correlation. The Cannonball scenario is also discussed and we find that this model cannot be excluded for GRB 060111B.